adsabs/AstroCLIMB huggingface dataset:
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Relative proton–electron heating (Q i/Q e) vs. ratio of the ion cyclotron time (τ  ci) to the nonlinear time (τ nl) evaluated at d i. For the MMS data, we identify −Π ij  D  ij  as the heating rate, ﹩{Q}_{s}=-{{\rm{\Pi }}}_{{ij}}^{s}{D}_{{ij}}^{s}﹩. Only intervals with positive ion and electron heating rates were considered. The two solid lines are parallel and have slopes of unity.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Comparison of the unperturbed GD-1 stream model (blue dots) and the observed GD-1 candidate stars in Malhan & Ibata (2019; red data points with error bar). On each panel, the horizontal axis is ϕ 1, while the vertical axis is ϕ 2, ϖ, v los, μ  α*, or μ  δ . As seen in the top right plot showing the (ϕ 1, v los) distribution, some of the GD-1 candidate stars are outlier (nonmember) stars with very different v los values. Apart from these outlier stars, our unperturbed GD-1 stream model reproduces the global properties of the observed GD-1 stream. We note that this unperturbed GD-1 stream model is used as a reference throughout this paper.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Relative proton–electron heating (Q i/Q e) vs. proton plasma beta, β p. Many data points from the 2.5D PIC simulation have the same β p, where the average Q i/Q e is shown.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Relative proton–electron heating (Q i/Q e) vs. the proton plasma beta (β p). The data points from various sources are compared with heating models proposed by Quataert (1998), Howes (2010), and Kawazura et al. (2019) for T i/T e = 1 and 6.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Schematic diagram for our simulations in this paper.
Paper: Turbulent Energy Transfer and Proton–Electron Heating in Collisionless Plasmas
Authors: S. Roy, R. Bandyopadhyay, Y. Yang, T. N. Parashar, W. H. Matthaeus, S. Adhikari, V. Roytershteyn, A. Chasapis, Hui Li, D. J. Gershman, B. L. Giles, J. L. Burch
Figure caption: Relative proton–electron heating (Q i/Q e) vs. c(β)τ ci/τ nl(d i).
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Morphology of the showcase GD-1 stream models NGC2808_698, NGC3201_202, and NGC5272_M3_261. Each model is displayed with three rows, and all horizontal axes are ϕ 1. The uppermost wide panel shows the 1D density ρ(ϕ 1) in our simulation (blue histogram) and in the observed data (de Boer et al. 2020; gray dashed line). The middle wide panel shows the full extent of the model stream in the (ϕ 1, ϕ 2) space. The lower five panels show the model stream near the gap region in the (ϕ 1, X) space, where X = ϕ 2, d, μ  α*, μ  δ , and v los from left to right. The red vertical lines surrounding the gap are the same for the upper and lower panels.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Illustration of how we compare the unperturbed model with a perturbed model. (a) Stellar distribution of the unperturbed model in the (ϕ 1, ϕ 2) space. (b) Histogram of the stellar distribution as a function of ϕ 1. This histogram is used as a proxy for the 1D density ρ unperturbed(ϕ 1). (c) Same as in panel (a), but for a perturbed model. (d) Same as in panel (c), but for the perturbed model. This histogram is used as a proxy for the 1D density ρ perturbed(ϕ 1). (e) Density ratio ρ perturbed/ρ unperturbed as a function of ϕ 1. The location of the minimum of this ratio (vertical gray line) is defined as the location of the gap, ϕ 1,gap. If the minimum ratio satisfies ρ perturbed/ρ unperturbed < 0.8 and the gap location satisfies −40° < ϕ 1,gap < 0°, we judge that the model has a GD-1-like gap.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Epoch of the close encounter with a GC (t encounter) and the location of the GD-1-like gap (ϕ 1,gap). We show all of the 57 simulations listed in Table 1. The 6 GCs with ﹩{P}_{\mathrm{gap}-\mathrm{forming}}\geqslant \tfrac{3}{1000}﹩ are marked by various symbols. The other 10 GCs are shown by gray, filled circles. The size of the symbol represents the strength of the gap. We note that the encounter with NGC5272 (M3) at t encounter ≃ −3.5 Gyr and that with IC4499 at t encounter ≃ −1.7 Gyr can form gaps at −40° < ϕ 1 < 0° and −20° < ϕ 1 < 0°, respectively.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: (a) Relationship between the mass and the gap-forming probability for the 16 GCs listed in Table 1. The six red dots are the GCs with ﹩{P}_{\mathrm{gap}-\mathrm{forming}}\geqslant \tfrac{3}{1000}﹩. (b) Normalized cumulative distribution for the mass of GCs with different ranges of P gap−forming. Those GCs with higher P gap−forming are typically more massive. Also, low-mass GCs (M GC ≲ 104.5 M ⊙) can hardly form a gap.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Additional simulations of the GD-1 stream model NGC2808_698 in which we used the particle spray method. In each simulation, we release the stars from the inner and outer Lagrange points with a constant stripping rate at −6 Gyr < t < t end. From top to bottom, we show the results with t end/ Gyr = −5, −4, −3, and −2. The left column corresponds to the simulations with no perturbation. The right column corresponds to the simulations with perturbation from NGC2808. The gap becomes clearer if the disruption ends at an earlier epoch.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Orbital properties of the GD-1 stream and GCs. (a) Azimuthal angular momentum and energy. (b) Apocentric and pericentric radii. The blue cross (+) corresponds to the GD-1 stream. The red dots correspond to the six GCs with ﹩{P}_{\mathrm{gap}-\mathrm{forming}}\geqslant \tfrac{3}{1000};﹩ among which two GCs (NGC5272 (M3) and IC4499) with the highest P gap−forming are highlighted with red ⊙. The black open circles correspond to the 10 GCs with ﹩0\lt {P}_{\mathrm{gap}-\mathrm{forming}}\leqslant \tfrac{2}{1000}﹩. The other GCs (namely, those GCs with P gap−forming = 0) are marked with gray dots.
Paper: Probability of Forming Gaps in the GD-1 Stream by Close Encounters of Globular Clusters
Authors: Yuka Doke, Kohei Hattori
Figure caption: Same as Figure 6, but for the showcase GD-1 stream models IC4499_311, FSR1758_731, and NGC7089_M2_138.
Paper: Observations of Rapidly Growing Whistler Waves in Front of Space Plasma Shock due to Resonance Interaction between Fluctuating Electron Velocity Distributions and Electromagnetic Fields
Authors: Jiansen He, Xingyu Zhu, Qiaowen Luo, Chuanpeng Hou, Daniel Verscharen, Die Duan, Wenya Li, Jinsong Zhao, Tieyan Wang, Daniel B. Graham, Qiugang Zong, Zhonghua Yao
Figure caption: The MMS spacecraft outside Earth’s bow shock observe an event of large-amplitude whistler waves. (a) Sketch of particles and waves measured by MMS in front of the bow shock. The elements displayed in order outward from the Earth at the center are the magnetic lines of the geo-magnetosphere (color coded with magnetic field strength), the bow shock (semitransparent purple surface), the four MMS satellites, and whistler waves (yellow curves). (b) Ion energy spectrum in a prolonged interval involving the outbound and inbound bow shock crossings. (c) Magnetic field components in the same prolonged interval. (d) Ion energy spectrum in a shorter subinterval but still including the event marked by the shaded area. (e) Magnetic field components in the same subinterval. (f) Electron energy spectrum in the same subinterval. (g) Electron temperatures (T e,∥, T e,⊥, and dimensional averaged T e) in the same subinterval. (h) Oscillations of the magnetic field (δ  B ) during the wave event. (i) Correlated oscillations of the electron fluid velocity (δ  V  e) during the wave event. (j) Weak oscillations of the ion fluid velocity (δ  V   i ) during the wave event. (k) Oscillations of the electric field in the ion mean bulk flow frame (﹩\delta {\boldsymbol{E}}^{\prime} ﹩) during the wave event. (l) Oscillations of the current density (δ  J ) during the wave event.
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption: Upper panel) From left to right in upper (CFHT g band) and lower (CFHT r band) segments: an image of I Zw 81, GALFIT best-fit model image, and corresponding residual image in magnitude units. The inset images in all images highlight the inner region of the galaxy. (Bottom panel) Isophotal surface brightness profile of the galaxy in CFHT g band. Solid black circles and red line show the observed and best-fit model profiles, respectively. The surface brightness distribution of the individual component is coded with different line styles and colors, as mentioned in the legends. The residual obtained by subtracting model surface brightness from that of the galaxy is shown in the lower segment of the bottom panel.
Paper: Observations of Rapidly Growing Whistler Waves in Front of Space Plasma Shock due to Resonance Interaction between Fluctuating Electron Velocity Distributions and Electromagnetic Fields
Authors: Jiansen He, Xingyu Zhu, Qiaowen Luo, Chuanpeng Hou, Daniel Verscharen, Die Duan, Wenya Li, Jinsong Zhao, Tieyan Wang, Daniel B. Graham, Qiugang Zong, Zhonghua Yao
Figure caption: Fundamental physics of field–particle interactions taking place in the foreshock region of planetary bow shock. The drift between solar-wind ions and shock-reflected ions in velocity space is intrinsically unstable and determines the dominant eigenmode together that transfers the free energy between fields and particles. Perturbations of the electromagnetic fields and the electron velocity distribution associated with this dominant eigenmode couple to drive the whistler waves, which then evolve into nonlinear large amplitude and may contribute to the reformation of shocklet and shock.
Paper: Observations of Rapidly Growing Whistler Waves in Front of Space Plasma Shock due to Resonance Interaction between Fluctuating Electron Velocity Distributions and Electromagnetic Fields
Authors: Jiansen He, Xingyu Zhu, Qiaowen Luo, Chuanpeng Hou, Daniel Verscharen, Die Duan, Wenya Li, Jinsong Zhao, Tieyan Wang, Daniel B. Graham, Qiugang Zong, Zhonghua Yao
Figure caption: Eigenmode instability driven by non-Maxwellian ion phase space density as predicted from linear theory of plasma kinetics. (a) Ion phase space density with the integrated multiorder moments of the two populations. This theoretical result is similar to the results of our ion observations. (b) Electron phase space density. The integrated multiorder moments are also similar to those of our observations. (c) Dispersion relation and (d) growth rate profile of right-hand polarized whistler waves based on the given ion and electron background velocity distributions. (e)–(h) Time sequences of the disturbed magnetic field vectors, electron bulk velocity vectors, electric field vectors, and current density vectors.
Paper: Observations of Rapidly Growing Whistler Waves in Front of Space Plasma Shock due to Resonance Interaction between Fluctuating Electron Velocity Distributions and Electromagnetic Fields
Authors: Jiansen He, Xingyu Zhu, Qiaowen Luo, Chuanpeng Hou, Daniel Verscharen, Die Duan, Wenya Li, Jinsong Zhao, Tieyan Wang, Daniel B. Graham, Qiugang Zong, Zhonghua Yao
Figure caption: Magnetic field and electron fluid velocity disturbances show right-handed polarization, which is typical for whistler waves. (a)–(b) Hodograms of the fluctuating magnetic field vectors (δ  B ) and the electron fluid velocity vectors (δ  V  e) in LMN coordinates as transformed from Geocentric Solar Ecliptic (GSE) coordinates through MVA. (c) Arrangement of fluctuating magnetic field vector (δ  B ) in chronological order.
Paper: Observations of Rapidly Growing Whistler Waves in Front of Space Plasma Shock due to Resonance Interaction between Fluctuating Electron Velocity Distributions and Electromagnetic Fields
Authors: Jiansen He, Xingyu Zhu, Qiaowen Luo, Chuanpeng Hou, Daniel Verscharen, Die Duan, Wenya Li, Jinsong Zhao, Tieyan Wang, Daniel B. Graham, Qiugang Zong, Zhonghua Yao
Figure caption: Evidence for ongoing enhancements of wave activity encountered by MMS. (a) Spectrum of ﹩\delta {\boldsymbol{J}}\cdot \delta {\boldsymbol{E}}^{\prime} ﹩ in a time–period diagram. (b) Spectrum of gamma, normalized growth rate, in the time–period diagram. (c) Frequency profiles of ﹩\delta {{\boldsymbol{J}}}_{{\rm{e}}}\cdot \delta {\boldsymbol{E}}^{\prime} ﹩ including the trace and the components in the parallel and perpendicular directions. (d) Frequency profiles of gamma (normalized energy conversion rate).
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Summed detection probabilities for all the 245 sources in our survey for which we can calculate masses. Red circles show the projected separation and estimated mass ratios for all detected companions. Red and yellow lines show the detection limits from our past surveys in Papers I and II, respectively. We use this map in Section 3.3 to model the separation and mass ratio distribution of the companion population in the ONC.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Corner plots representing the posterior distributions of the four- and three-parameter models used in our fit to the companion population. Beta_q is the exponent to the power-law model of the mass ratio distribution, CF is the companion frequency over q = 0–1 and a = 10–200 au, log(a_o) is the mean of the log-normal separation distribution used in the four-parameter model, sigma_log(a) is the standard deviation of the log-normal separation distribution used in the four-parameter model, and Beta_a is the power-law exponent to the separation distribution used in the three-parameter model. The separation distribution is unconstrained with a log-normal, likely due to the limited range of our survey. Evidence values show no statistical preference between the three- and four-parameter models, and therefore we use the three-parameter model fits for further analysis.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Color–magnitude diagram for all the sources that were included in our sample with F435W and F555W data. The detected binaries are plotted with both the primary and secondary components. The solid lines are the BT-Dusty 1–3 Myr isochrones with specific masses chosen for reference. The black dashed line represent the extinction vector derived from Cardelli et al. (1989).
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: Each line shows the 0.1% false-positive probability line associated with our double-PSF fitting routine for the listed S/N in the F435W filter on HST/ACS, adapted from Paper II.
Paper: Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: Matthew De Furio, Christopher Liu, Michael R. Meyer, Megan Reiter, Adam Kraus, Trent Dupuy, John Monnier
Figure caption: The J – H vs. H – K color–color plot for the sources with detected companions within our survey (black circles), showing no obvious signs of disk excess. Overplotted are the observed pre-main-sequence (PMS) and main-sequence (MS) colors of Pecaut & Mamajek (2013, PM13), the reddening vector (Cardelli et al. 1989), and the classical T-Tauri star (CTTS) locus from Meyer et al. (1997).
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Light curve of Gaia19fct. ZTF (g, r; Masci et al. 2019), HOYS (V, R, I; Froebrich et al. 2018; Evitts et al. 2020), WISE (W1 and W2; Mainzer et al. 2011), 2MASS (J, H, K  s ; Cutri et al. 2003), UKIDSS (J, H, K  s ; Lawrence et al. 2007), Pan-STARRS (g, r, i, z, y; Chambers et al. 2016), and Gaia archives (G), as well as our RC80 (g, V, r, i) and REM (J, H, K  s ) monitoring observation data, are used. Circles and stars represent public domain data and our observations, respectively. Black dashed and dashed–dotted lines indicate IGRINS and NOTCam spectral observing dates, respectively. Uncertainties smaller than the symbol size are not presented.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: This figure illustrates the relative contribution of five underlying factors to the derived measurement error of a planet’s density. The x-axis represents a minimum amount that a given parameter contributes to the overall uncertainty on density. Solid colored lines represent directly observable quantities (period, transit depth, and RV amplitude), while dashed colored lines refer to model-dependent quantities (stellar mass and radius). The black line (“shape”) shows the ratio of tidally induced variation to measurement error (Δ ρ /σ  ρ ). The gray line shows a similar value after having artificially reduced the overall uncertainty on density by a factor of 3 to highlight the effect of future measurement improvements.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: Mass–radius relationships along with data points (and error bars) for the sample of planets considered in this work. The left and right panels refer to low- and high-mass planets, respectively. Black curves in the left panel are taken from Zeng et al. (2019). Colored bands represent variations of these curves by up to 4.7% in radius, corresponding to density variations of up to 15%. The right panel shows a similar phenomenon for high-mass planets, where we show constant–density relations corresponding to solar system gas giant densities, as well as a planet with half the density of Saturn and a planet with a density of 0.2 g cm−3 representative of “super puffs.” The planets highlighted in red are those mentioned in Table 2 whose density uncertainty is less than the deviations caused by tides.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: SED of Gaia19fct. Different colors and symbols present different epochs. For the 2018–2019 period, we used the ZTF gr and REM JHK  s  observed in 2018 November and August, respectively, and NEOWISE W1 and W2 observed in 2019 March. For the 2021–2022 period, we adopted the RC80 gVri, Gaia G, and REM JHK  s  observed in 2022 February and NEOWISE W1 and W2 obtained in 2021 March.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: The factor by which the uncertainty on a planet’s density needs to be improved such that it is equal to the change in density due to tidal deformations. The dashed black line highlights a decrease by a factor of 3 in the uncertainty on spherical planet density. The orange region highlights planets whose density uncertainty is currently less than the difference between the spherical and tidal density values.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: Relative change in the density of planets with orbital periods less than 3 days. The curves show the functional dependence of Equation (8) for representative values of planet mass and radius.
Paper: Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: David Berardo, Julien de Wit
Figure caption: We show here agreement between the functional form of the density perturbation we derive in Section 3.2.2 (x-axis) against the values calculated in Section 3.2.1 (y-axis). The black line shows a linear relationship with a slope of 2 passing through the origin. The coloring represents the mass of each planet on a log scale.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Pan-STARRS giy color-composite image of Gaia19fct. The image shows a 1′ × 1′ area centered on Gaia19fct, and the companion is located 2″ to the west.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: Confusion matrix from withheld test set for all models. The x-axis is the percentage of disks in that class that were predicted accordingly. (a) Using a 50% decision threshold. (b) Using a 75% decision threshold. (c) Using a 90% decision threshold. (d) Using a 95% decision threshold. The top left and bottom right blocks of each panel show the counts of true negatives and true positives, respectively. The top right and bottom left blocks of a panel show the false positives and false negatives, respectively. A perfectly accurate model will have no entries in the top right and bottom left.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: Left: various metrics calculated from the withheld test set for all models. Right: corresponding receiver operating characteristic (ROC) curves. Error bars show 95% confidence intervals that are calculated by bootstrapping each metric 1000 times using random selections of 80% of the test data. The percentages next to the accuracy labels denote the decision threshold.